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Fig. 2.


Left: surface brightness map (in MJy sr−1) of PACS 100 μm in the junction region. The colour scale is cut to reveal the cloud structure because the brightest source (s1446) peaks over 60 000 MJy sr−1. The red contours show the integrated emission of N2H+ at 1, 2, 3, 4, and 5 K km s−1. The yellow ellipses show the FWHM of the GCC sources, whose ID numbers are written in black. Right: three columns show for sources 1446, 1449, and 1458 the source SED, its Tdust profile, and maps of WISE 3.4 μm, WISE 12 μm, PACS 100 μm, and SPIRE 250 μm bands. In the SEDs, blue diamonds are 2MASS J, H, and Ks fluxes from the 2MASS PSC. Green upward-pointing triangles are Spitzer 3.6, 4.5, 5.8, 8.0, and 24 μm fluxes from the YSO catalogue of Renaud et al. (2013). Green downward-pointing triangles are WISE 3.4, 4.6, 12, and 22 μm fluxes from our photometry measurements. Orange diamonds are AKARI 9, 18, 65, 90, 140, and 160 μm fluxes from the AKARI MIR and FIR point source catalogues. Red squares show the fluxes of PACS 100 and 160 μm from our photometry measurements. Black circles are fluxes of PACS 160 and SPIRE 250, 350, and 500 μm from the GCC catalogue of compact sources. For the fluxes selected from public point source catalogues, we considered only the source nearest to the GCC source centre. The source number in the GCC catalogue is indicated in the top left corner of the SED plot, as is the final classification (SL = starless, PS = protostellar, 1 = candidate, and 2 = confirmed). In the Tdust profiles, the black points are individual pixels, the blue lines show the background Tdust, the red lines are Gaussian fits, and the grey area shows the 1σ fit uncertainties.

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